Data di Pubblicazione:
2014
Abstract:
This paper describes the methods used to produce photometrically
calibrated maps from the Planck High Frequency Instrument (HFI) cleaned,
time-ordered information. HFI observes the sky over a broad range of
frequencies, from 100 to 857 GHz. To obtain the best calibration
accuracy over such a large range, two different photometric calibration
schemes have to be used. The 545 and 857 GHz data are calibrated by
comparing flux-density measurements of Uranus and Neptune with models of
their atmospheric emission. The lower frequencies (below 353 GHz) are
calibrated using the solar dipole. A component of this anisotropy is
time-variable, owing to the orbital motion of the satellite in the solar
system. Photometric calibration is thus tightly linked to mapmaking,
which also addresses low-frequency noise removal. By comparing
observations taken more than one year apart in the same configuration,
we have identified apparent gain variations with time. These variations
are induced by non-linearities in the read-out electronics chain. We
have developed an effective correction to limit their effect on
calibration. We present several methods to estimate the precision of the
photometric calibration. We distinguish relative uncertainties (between
detectors, or between frequencies) and absolute uncertainties. Absolute
uncertainties lie in the range from 0.54% to 10% from 100 to 857 GHz. We
describe the pipeline used to produce the maps from the HFI timelines,
based on the photometric calibration parameters, and the scheme used to
set the zero level of the maps a posteriori. We also discuss the
cross-calibration between HFI and the SPIRE instrument on board
Herschel. Finally we summarize the basic characteristics of the set of
HFI maps included in the 2013 Planck data release.
calibrated maps from the Planck High Frequency Instrument (HFI) cleaned,
time-ordered information. HFI observes the sky over a broad range of
frequencies, from 100 to 857 GHz. To obtain the best calibration
accuracy over such a large range, two different photometric calibration
schemes have to be used. The 545 and 857 GHz data are calibrated by
comparing flux-density measurements of Uranus and Neptune with models of
their atmospheric emission. The lower frequencies (below 353 GHz) are
calibrated using the solar dipole. A component of this anisotropy is
time-variable, owing to the orbital motion of the satellite in the solar
system. Photometric calibration is thus tightly linked to mapmaking,
which also addresses low-frequency noise removal. By comparing
observations taken more than one year apart in the same configuration,
we have identified apparent gain variations with time. These variations
are induced by non-linearities in the read-out electronics chain. We
have developed an effective correction to limit their effect on
calibration. We present several methods to estimate the precision of the
photometric calibration. We distinguish relative uncertainties (between
detectors, or between frequencies) and absolute uncertainties. Absolute
uncertainties lie in the range from 0.54% to 10% from 100 to 857 GHz. We
describe the pipeline used to produce the maps from the HFI timelines,
based on the photometric calibration parameters, and the scheme used to
set the zero level of the maps a posteriori. We also discuss the
cross-calibration between HFI and the SPIRE instrument on board
Herschel. Finally we summarize the basic characteristics of the set of
HFI maps included in the 2013 Planck data release.
Tipologia CRIS:
1.1 Articolo in rivista
Keywords:
cosmic background radiation; cosmology: observations; surveys; methods: data analysis
Elenco autori:
P., Collaboration; P. A., R.; N., Aghanim; C., Armitage Caplan; M., Arnaud; M., Ashdown; F., Atrio Barandela; J., Aumont; C., Baccigalupi; A. J., Banday; R. B., Barreiro; E., Battaner; K., Benabed; A., Beno�t; A., Benoit L�vy; J., Bernard; M., Bersanelli; B., Bertincourt; P., Bielewicz; J., Bobin; J. J., Bock; J. R., Bond; J., Borrill; F. R., Bouchet; F., Boulanger; M., Bridges; M., Bucher; C., Burigana; J., Cardoso; A., Catalano; A., Challinor; A., Chamballu; R., Chary; X., Chen; H. C., Chiang; L., Chiang; P. R., Christensen; S., Church; D. L., Clements; S., Colombi; L. P., L.; C., Combet; F., Couchot; A., Coulais; B. P., Crill; A., Curto; F., Cuttaia; L., Danese; R. D., Davies; P. d., Bernardis; A. d., Rosa; G. d., Zotti; J., Delabrouille; J., Delouis; F., D�sert; C., Dickinson; J. M., Diego; H., Dole; S., Donzelli; O., Dor�; M., Douspis; X., Dupac; G., Efstathiou; T. A., En�lin; H. K., Eriksen; C., Filliard; F., Finelli; O., Forni; M., Frailis; E., Franceschi; S., Galeotta; K., Ganga; M., Giard; G., Giardino; Y., Giraud H�raud; J., Gonz�lez Nuevo; K. M., G�rski; S., Gratton; A., Gregorio; A., Gruppuso; F. K., Hansen; D., Hanson; D., Harrison; G., Helou; S., Henrot Versill�; C., Hern�ndez Monteagudo; D., Herranz; S. R., Hildebrandt; E., Hivon; M., Hobson; W. A., Holmes; A., Hornstrup; W., Hovest; K. M., Huffenberger; A. H., Jaffe; T. R., Jaffe; W. C., Jones; M., Juvela; E., Keih�nen; R., Keskitalo; T. S., Kisner; R., Kneissl; J., Knoche; L., Knox; M., Kunz; H., Kurki Suonio; G., Lagache; J., Lamarre; A., Lasenby; R. J., Laureijs; C. R., Lawrence; M. L., Jeune; E., Lellouch; R., Leonardi; C., Leroy; J., Lesgourgues; M., Liguori; P. B., Lilje; M., Linden V�rnle; M., L�pez Caniego; P. M., Lubin; J. F., Mac�as P�rez; B., Maffei; N., Mandolesi; M., Maris; D. J., Marshall; P. G., Martin; E., Mart�nez Gonz�lez; S., Masi; M., Massardi; S., Matarrese; F., Matthai; L., Maurin; P., Mazzotta; P., Mcgehee; P. R., Meinhold; A., Melchiorri; L., Mendes; A., Mennella; M., Migliaccio; S., Mitra; M., Miville Desch�nes; A., Moneti; L., Montier; R., Moreno; G., Morgante; D., Mortlock; D., Munshi; J. A., Murphy; P., Naselsky; F., Nati; P., Natoli; C. B., Netterfield; H. U., N�rgaard Nielsen; F., Noviello; D., Novikov; I., Novikov; S., Osborne; C. A., Oxborrow; F., Paci; L., Pagano; F., Pajot; R., Paladini; D., Paoletti; B., Partridge; F., Pasian; G., Patanchon; T. J., Pearson; O., Perdereau; L., Perotto; F., Perrotta; F., Piacentini; M., Piat; E., Pierpaoli; D., Pietrobon; S., Plaszczynski; E., Pointecouteau; G., Polenta; N., Ponthieu; L., Popa; T., Poutanen; G. W., Pratt; G., Pr�zeau; S., Prunet; J., Puget; J. P., Rachen; M., Reinecke; M., Remazeilles; C., Renault; S., Ricciardi; T., Riller; I., Ristorcelli; G., Rocha; C., Rosset; G., Roudier; B., Rusholme; D., Santos; G., Savini; D., Scott; E. P., S.; L. D., Spencer; J., Starck; V., Stolyarov; R., Stompor; R., Sudiwala; R., Sunyaev; F., Sureau; D., Sutton; A., Suur Uski; J., Sygnet; J. A., Tauber; D., Tavagnacco; S., Techene; Terenzi, Luca; M., Tomasi; M., Tristram; M., Tucci; G., Umana; L., Valenziano; J., Valiviita; B. V., Tent; P., Vielva; F., Villa; N., Vittorio; L. A., Wade; B. D., Wandelt; D., Yvon; A., Zacchei; A., Zonca
Link alla scheda completa:
Pubblicato in: